2013A&A...558A.107G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST02:53:57

2013A&A...558A.107G - Astronomy and Astrophysics, volume 558A, 107-107 (2013/10-1)

Magnetohydrodynamics of Mira's cometary tail.

GOMEZ E.A.

Abstract (from CDS):

The asymptotic giant-branch, long-period variable star Mira exhibits a 4 parsec long cometary tail in the far-ultraviolet. We address the issue of the origin of this structure and its emission process by simulating the transition of this star from the interstellar medium to the Local Bubble, which is a tenuous, high-pressure medium. We use the hydrodynamic and the magnetohydrodynamic modules of the PLUTO astrophysical code to carry out our simulations. We study the system without a cooling function, with a simplified exponential cooling function, and with a simplified nonequilibrium cooling function. We find evidence that magnetohydrodynamics constrain the shape of the cometary tail and explain features of its far-ultraviolet emission. We suggest an emission process that involves C0 excitation through inelastic electron collisions and a two-photon continuum to explain the luminosity of Mira's tail.

Abstract Copyright:

Journal keyword(s): radiation mechanisms: thermal - stars: AGB and post-AGB - ISM: magnetic fields - methods: numerical - waves - ISM: jets shock, outflows

Simbad objects: 5

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Number of rows : 5

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 SH 2-188 PN 01 30 33.1777443823 +58 24 50.324516367   17.424 17.447 17.398 17.376 DAO.6 91 1
2 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1434 0
3 * omi Cet B WD* 02 19 20.80 -02 58 40.0           DA 39 1
4 NGC 1265 GiC 03 18 15.674 +41 51 27.94   14.7       ~ 349 2
5 NAME Local Bubble ISM ~ ~           ~ 693 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-02:53:57

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